TRUWIZ 123a

 September 09 2022: 

                                                      TRUWIZ 123a            

(see also truwiz123b)

trusciencetrutechnology@blogspot.com

Volume 2022, Dated: 09 September 2022

[Initiated by Prof. Dr. K. Lakshmi Narayana]

In Memory of

Late Professor Kotcherlakota Rangadhama Rao

                                                                     D.Sc. (Madras).a D.Sc. (London).

(Birth on 09 September 1899 Early Morning, Berhampur, Demise on 20 June 1972 at 9 h 09 m at Visakhapatnam), at his residence, Narasimha Ashram, Official Colony, Maharanipeta. P. O., Visakhapatnam 530002. [Mrs. Peramma Rangadhama Rao demise on 31 Dec 1971 around 10 AM. at Narasimha Ashram, Official Colony, Maharanipeta.P.O.Visakhapatnam.]

                       TRUWIZ-123a

Q1. arXiv:2110.02227 [astro-ph.HE]: Tue, 5 Oct 2021 18:00:01 UTC (29,807 KB): [Submitted on 5 Oct 2021]: Jets in Common Envelopes: a low mass main sequence star in a red giant. Diego Lopez-Camara, Fabio De Colle, Enrique Moreno Mendez, Sagiv Shiber, Roberto Iaconi. :ABSTRACT: We present small scale three dimensional hydrodynamical simulations of the evolution of a 0.3Msun main sequence star which launches two perpendicular jets within the envelope of a 0.88Msun red giant. Based on the large scale simulations of Shiber et al. (2019), we study the dynamics of the jets either when the secondary star is grazing the envelope of the red giant, or when it has plunged-in the envelope. The dynamics of the jets through the common envelope (CE) depend on the conditions of the environment as well as on the jet power. Jets are successful in removing the envelope during the early grazing envelope phase and the initial plunge-in CE phases. Deep inside the CE, the jets are drowned. High luminosity emission going from X-rays to UV and optical is expected when the jets break out of the CE. We find that the mass accretion onto the MS star is 1-10\% of the Bondi Hoyle Littleton rate. The amount of angular momentum accreted on to the secondary is not large enough to form a disk. Our study shows the benefits of coupling large scale models with small scale as the global evolution can critically depend on the small scale 

                       a. envelops    b. phenomena     c. drowned    d. conditions.

Q2. arXiv:2110.02250 [astro-ph.GA]:  Tue, 5 Oct 2021 18:03:59 UTC (4,115 KB): [Submitted on 5 Oct 2021]: Measuring chemical likeness of stars with RSCA, Damien de Mijolla, Melissa K. Ness. ABSTRACT: Identification of chemically similar stars using elemental abundances is core to many pursuits within Galactic archaeology. However, measuring the chemical likeness of stars using abundances directly is limited by systematic imprints of imperfect synthetic spectra in abundance derivation. We present a novel data-driven model that is capable of identifying chemically similar stars from spectra alone. We call this Relevant Scaled Component Analysis (RSCA). RSCA finds a mapping from stellar spectra to a representation that optimizes recovery of known open clusters. By design, RSCA amplifies factors of chemical abundance variation and minimizes those of non-chemical parameters, such as instrument systematics. The resultant representation of stellar spectra can therefore be used for precise measurements of chemical similarity between stars. We validate RSCA using 185 cluster stars in 22 open clusters in the APOGEE survey. We quantify our performance in measuring chemical similarity using a reference set of 151,145 field stars. We find that our representation identifies known stellar siblings more effectively than stellar abundance measurements. Using RSCA, 1.8% of pairs of field stars are as similar as birth siblings, compared to 2.3% when using stellar abundance labels. We find that almost all of the information within spectra leveraged by RSCA fits into a two-dimensional basis, which we link to [Fe/H] and alpha-element abundances. We conclude that chemical tagging of stars to their birth clusters remains prohibitive. However, using the spectra has noticeable gain, and our approach is poised to benefit from larger datasets and improved algorithm 

                              a designs     b. practicals     c. benefits    d. labels.

Q3.arXiv:2110.02347 [astro-ph.HE]: Tue, 5 Oct 2021 20:30:30 UTC (4,905 KB)[Submitted on 5 Oct 2021]: Triangulating Black Hole Forming Stellar Collapses through Neutrinos. Lila Sarfati, Rasmus S. L. Hansen, Irene Tamborra. :ABSTRACT: In the event of a black hole (BH) forming stellar collapse, the neutrino signal should terminate abruptly at the moment of BH formation, after a phase of steady accretion. Since neutrinos are expected to reach Earth hours before the electromagnetic signal, the combined detection of the neutrino burst through multiple neutrino telescopes could allow to promptly determine the angular location of a nearby stellar collapse in the sky with high precision. In this paper, we contrast the triangulation pointing procedure that relies on the rise time of the neutrino curve, often considered in the literature, to the one that takes advantage of the cutoff of the neutrino curve at the moment of BH formation. By forecasting the neutrino signal expected in the IceCube Neutrino Observatory, Hyper-Kamiokande and DUNE, we devise a strategy to optimize the identification of the rise and cutoff time of the neutrino curve. We show that the triangulation method developed by employing the end tail of the neutrino curve allows to achieve at least one order of magnitude improvement in the pointing precision for a galactic burst, while being insensitive to the neutrino mixing scenario. The triangulation pointing method based on the cutoff of the neutrino curve will also guarantee a better performance for BH forming collapses occurring beyond our own 

                      a. supernove    b. planets    c. neutrinos    d.  Galaxy.

Q4.arXiv:2110.02354 [astro-ph.SR]: Tue, 5 Oct 2021 20:49:58 UTC (911 KB): [Submitted on 5 Oct 2021]: Review of the Classification and Properties of 40 Variable Stars in Sagittarius. G. Agli'  et al.,  Italy. ABSTRACT: This study aims to assess the properties and classification of 40 variable stars in Sagittarius, little studied since their discovery and reported in the Information Bulletin on Variable Stars (IBVS) 985 and update. Using data from previous studies and several astronomical databases, we performed our analysis mainly utilizing a period analysis software and comparing the photometric characteristics of the variables in a Colour-Absolute Magnitude Diagram. For all stars, the variability is confirmed. We discovered new significant results for the period and/or type of 15 variables and highlighted incorrect cross-reference names on astronomical databases for 5 stars. This assessment also identifies 9 cases for which results from the ASAS-SN Catalog of Variable Stars are systematically not consistent with the original light curves. A correct identification of NSV 10522 is 

                                a. amazed   b. discussed  c.provided    d. elaborated.

Q5.arXiv:2110.02996 [astro-ph.HE]: Wed, 6 Oct 2021 18:12:35 UTC (402 KB)[Submitted on 6 Oct 2021]:Testing extended theories of gravity with GRBs. L. Mastrototaro, G. Lambiase. :ABSTRACT:We present our studies on the neutrino pairs annihilation into electron-positron pairs (νν¯→e−e+) near the surface of a neutron star in the framework of extended theories of gravity. The latter modifies the maximum energy deposition rate near to the photonsphere and it might be several orders of magnitude greater than that computed in the framework of General Relativity. These results provide a rising in the Gamma-Ray Bursts energy emitted from a close binary neutron star system and might be a fingerprint of modified theories of gravity, changing our view of astrophysical 

                                 a. criteria   b. phenomena   c. theory   d. review.

Q6.arXiv:2110.03601 [astro-ph.SR]: Thu, 7 Oct 2021 16:25:11 UTC (955 KB):

[Submitted on 7 Oct 2021]: Anomalous Cosmic Ray Oxygen Observations in to 0.1 au.

Jamie S. Rankin, et al., :ABSTRACT: The Integrated Science Investigation of the

Sun instrument suite onboard NASA's Parker Solar Probe mission continues to

measure solar energetic particles and cosmic rays closer to the Sun than

ever before. Here, we present the first observations of cosmic rays into 0.1 au

(21.5 solar radii), focusing specifically on oxygen from ~2018.7 to ~2021.2.

Our energy spectra reveal an anomalous cosmic ray-dominated profile that is

comparable to that at 1 au, across multiple solar cycle minima. The galactic

cosmic ray-dominated component is similar to that of the previous solar minimum

(Solar Cycle 24/25 compared to 23/24) but elevated compared to the past

(Solar Cycle 20/21). The findings are generally consistent with the current trend of

unusually weak solar modulation that originated during the previous solar minimum

and continues today. We also find a strong radial intensity gradient: 49.4 +/- 8.0 %/au

from 0.1 to 0.94 au, for energies of 6.9 to 27 MeV/nuc. This value agrees with that

measured by Helios nearly 45 years ago from 0.3 to 1.0 au (48 +/- 12 %/au;

9 to 29 MeV/nuc) and is larger than predicted by models. The large ACR gradients

observed close to the Sun by the Parker Solar Probe Integrated Science Investigation

of the Sun instrument suite found here suggest that intermediate-scale variations

in the magnetic field's structure strongly influences cosmic ray drifts, well inside

a 0.1au b. 1au c 2au d. 0.01au Q7. arXiv:2110.03658 [astro-ph.GA]: Thu, 7 Oct 2021 17:51:05 UTC (6,440 KB):

[Submitted on 7 Oct 2021]: The Milky Way's middle aged inner ring. Shola M. Wylie,

Jonathan P. Clarke, Ortwin E. Gerhard: ABSTRACT:We investigate the metallicity, age,

and orbital anatomy of the inner Milky Way specifically focussing on the outer bar

region. We integrate a sample of APOGEE DR16 inner Galaxy stars in a state of the

art bar-bulge potential with a slow pattern speed and investigate the link between

the resulting orbits and their [Fe/H] and ages. By superimposing the orbits we build

density, [Fe/H], and age maps of the inner Milky Way, which we divide further using

the orbital parameters eccentricity, |Xmax|, and |Zmax|. We find that at low heights

from the Galactic plane the Galactic bar gradually transitions into a radially thick,

vertically thin, elongated inner ring with average solar [Fe/H]. This inner ring is mainly

composed of stars with AstroNN ages between 4 and 9 Gyr with a peak in age between

6 and 8 Gyr, making the average age of the ring ~6 Gyr. The vertical thickness of the

ring decreases markedly towards younger ages. We also find very large L4 Lagrange

orbits that have average solar to super-solar metallicities and intermediate ages.

Lastly, we confirm a clear X-shape in the [Fe/H] and density distributions at large

Galactic heights. The orbital structure obtained for the APOGEE stars reveals that the

Milky Way hosts an inner ring-like structure between the planar bar and corotation.

This structure is on average metal rich, intermediately aged, and enhances the

horizontal gradient along the bar's a. minor axis b. lower axis c.major axis d. upper axis. Q8. arXiv:2110.03236 [physics.plasm-ph]:Thu, 7 Oct 2021 07:42:35 UTC (253 KB):

[Submitted on 7 Oct 2021]: A Modern-day Alchemy: Double Glow Plasma Surface

Metallurgy Technology. Zhong Xu, et al., :ABSTRACT: In the long history of science

and technology development, one goal is to diffuse solid alloy elements into the

surface of steel materials to form surface alloys with excellent physical and chemical

properties. On the basis of plasma nitriding technology, double glow plasma surface

technology has answered this challenge. This technology, which seems to be a

modern-day alchemy, can use any element in the periodic table of chemical elements,

including solid metal elements and their combinations, to form many types of surface

alloyed layers with high hardness, wear resistance, corrosion resistance and high

temperature oxidation resistance on various metal materials. For examples, nickel

base alloys, stainless steels and high speed steels are formed on the surfaces of

ordinary carbon steels; and high hardness, wear resistance and high temperature

oxidation resistance alloy are formed on the surface of titanium alloy.This article

briefly introduces the formation and principle of double glow plasma surface

metallurgy technology, and summarizes the experimental results and industry

application. The significance and development prospect of this technology are a. discussed b. presented c. enumerated d. dealtwith.

Q9.arXiv:2110.03000 [gr-qc]:  Wed, 6 Oct 2021 18:17:54 UTC (2,897 KB): [Submitted on 6 Oct 2021]: Self-interactions can stabilize excited boson stars. Nicolas Sanchis-Gual, Carlos Herdeiro, Eugen Radu. : ABSTRACT: We study the time evolution of spherical, excited (i.e. nodeful) boson star models. We consider a model including quartic self-interactions, controlled by a coupling Λ. Performing non-linear simulations of the Einstein-(complex)-Klein-Gordon system, using as initial data equilibrium boson stars solutions of that system, we assess the impact of Λ in the stability properties of the boson stars. In the absence of self-interactions (Λ=0), we observe the known behaviour that the excited stars in the (candidate) stable branch decay to a non-excited star without a node; however, we show that for large enough values of the self-interactions coupling, these excited stars do not decay (up to timescales of about t∼10^4). The stabilization of the excited states for large enough self-interactions is further supported by evidence that the nodeful states dynamically form through the gravitational cooling mechanism, starting from dilute initial data. Our results support the healing power (against dynamical instabilities) of self-interactions, recently unveiled in the context of the non-axisymmetric instabilities of spinning boson 

                                              a. interactions   b. giants    c. stars    d. systems.

Q10. arXiv:2110.03182 [gr-qc]: Thu, 7 Oct 2021 04:57:54 UTC (826 KB): [Submitted on 7 Oct 2021]: Quark stars in 4-dimensional Einstein-Gauss-Bonnet gravity. Ksh. Newton Singh, S. K. Maurya, Abhisek Dutta, Farook Rahaman, Somi Aktar:ABSTRACT: The article explores the first exact solution in a four-dimensional EGB-gravity with an anisotropic matter source. The solution has been found by two assumptions, a metric potential and the MIT-bag equation of state. Further, the solution has been tested with several physical constraints. Finally, using the boundary condition we have also estimated the range of bag constant B by varying the mass of the structure and the Gauss-Bonnet coupling constant α. This allows us to check the physical viability of the solution by comparing it with the existing accepted range of bag constant B.

       a. bag constant B  b. bag constant C  c. Bag constant F   d. bag constant E.

 Q11. arXiv:2110.03428 [gr-qc]:  Wed, 6 Oct 2021 00:27:23 UTC (4,188 KB)[Submitted on 6 Oct 2021]: Dynamical Friction From Ultralight Dark Matter. Yourong Wang, Richard Easther. :ABSTRACT: We simulate the gravitational dynamics of a massive object interacting with Ultralight / Fuzzy Dark Matter (ULDM/FDM), non-relativistic quantum matter described by the Schrodinger-Poisson equation. We first consider a point mass moving in a uniform background, and then a supermassive black hole (SMBH) moving within a ULDM soliton. After replicating simple dynamical friction scenarios to verify our numerical strategies, we demonstrate that the wake induced by a moving mass in a uniform medium may undergo gravitational collapse that dramatically increases the drag force, albeit in a scenario unlikely to be encountered astrophysically. We broadly confirm simple estimates of dynamical friction timescales for a black hole at the center of a halo but see that a large moving point mass excites coherent "breathing modes" in a ULDM soliton. These can lead to "stone skipping" trajectories for point masses which do not sink uniformly toward the center of the soliton, as well as stochastic motion near the center itself. These effects will add complexity to SMBH-ULDM interactions and to SMBH mergers in a ULDM 

                             a. galaxy   b. friction     c. center     d. universe.

Q12. arXiv:2110.03365 [hep-ph]: Thu, 7 Oct 2021 12:03:30 UTC (112 KB): [Submitted on 7 Oct 2021]: Probing light dark matter particles with astrophysical experiments. Tanmay Kumar Poddar. :ABSTRACT: The evidence of gravitational wave was first indirectly confirmed by the orbital period loss of Hulse-Taylor binary system which agrees well with the Einstein's general relativistic prediction. The perihelion precession of planets, gravitational light bending and Shapiro time delay are other tests of Einstein's general theory of relativity. However there are small uncertainties in the measurements of those observations from the general relativistic prediction. To account those uncertainties, we propose radiation of ultralight axions and vector gauge boson particles in the context of U(1)′ extended beyond standard model scenario. We obtain constraints on ultralight axion parameters (axion mass and decay constant) from the observational uncertainties of orbital period loss of compact binary systems, gravitational light bending, Shapiro time delay and birefringence phenomena. We also obtain the bounds on ultralight U(1)Lμ−Lτ gauge bosons from the orbital period loss of compact binary systems. The uncertainties in the perihelion precession of planets also put bounds on the U(1)Le−Lμ,τ light gauge bosons. These light particles can be promising candidates of fuzzy dark matter which can be probed from the above precision measurements.

                        a.  data      b. measurements    c. experiments    d. analysis.

Q13. arXiv:2110.06950 [astro-ph.GA]: (or arXiv:2110.06950v1 [astro-ph.GA] for this version): : [Submitted on 13 Oct 2021]: S5: The Orbital and Chemical Properties of One Dozen Stellar Streams. Ting S. Li, et al., : ABSTRACT: We report the kinematic, orbital, and chemical properties of 12 stellar streams with no evident progenitors, using line-of-sight velocities and metallicities from the Southern Stellar Stream Spectroscopic Survey (S^5), proper motions from Gaia EDR3, and distances derived from distance tracers or the literature. This data set provides the largest homogeneously analyzed set of streams with full 6D kinematics and metallicities. All streams have heliocentric distances between ∼10−50 kpc. The velocity and metallicity dispersions show that half of the stream progenitors were dwarf galaxies (DGs), while the other half originated from disrupted globular clusters (GCs). Based on the mean metallicities of the streams and the mass-metallicity relation, the luminosities of the progenitors of the DG streams range between Ursa Major I and Carina (−9.5≲MV≲−5.5). Four of the six GC streams have mean metallicities of [Fe/H] <−2, more metal-poor than typical Milky Way (MW) GCs at similar distances. Interestingly, the 300S and Jet GC streams are the only streams on retrograde orbits in our dozen stream sample. Finally, we compare the orbital properties of the streams with known DGs and GCs in the MW, finding several possible associations. Some streams appear to have been accreted with the recently discovered Gaia-Enceladus-Sausage system, and others suggest that GCs were formed in and accreted together with the progenitors of DG streams whose stellar masses are similar to Draco to ----------- (∼10^5−10^6M⊙).

                     a. compton      b. supernova   c. milkyway    d. Carina.

Q14.arXiv:2110.06995 [astro-ph.GA]: (or arXiv:2110.06995v1 [astro-ph.GA] for this version): [Submitted on 13 Oct 2021]: Deep Chandra observations of diffuse hot plasma in M83. Authors. Q. Daniel Wang, Yuxuan Zeng, Akos Bogda, Li Ji: :ABSTRACT: It is widely believed that galaxy formation and evolution is regulated by stellar mechanical feedback in forms of fast stellar winds and supernova explosions. However, the coupling of this feedback with the interstellar medium remains poorly understood. We examine how the coupling may be traced by diffuse soft X-ray emission in M83 -- a nearby face-on spiral galaxy undergoing active star formation, based chiefly on 729~ks Chandra observations. Our main findings are 1) the X-ray emission is enhanced not only along the galaxy's grand spiral arms, but also clearly in their downstreams; 2) the spectrum of the emission can be well characterized by a super-solar metallicity plasma with a lognormal temperature distribution, plus an X-ray absorption of a lognormal column density distribution; 3) the intensity of the emission is strongly anti-correlated with the dust obscuration seen in optical images of the galaxy. These findings suggest A) the morphology of the X-ray emission is likely due to the convolution of the feedback heating of the plasma with its thermal and dynamical evolution; B) the X-ray emission, accounting for ~10% of the feedback energy input rate, probably traces only the high-energy tail of the radiation from the plasma; C) a good fraction of the recent star forming regions seems sufficiently energetic to produce multi-phased outflows, likely responsible for much of the dust obscuration and X-ray absorption. Direct confrontation of the findings with theories/simulations could help to understand the underlying astrophysics of the coupling and how the hot plasma shapes the interstellar 

                                   a medium   b. space    c. plasma   d. energy.

Q15. arXiv:2110.07164 [astro-ph.HE]: Thu, 14 Oct 2021 06:00:48 UTC (1,062 KB): [Submitted on 14 Oct 2021]: AT2018lqh: Black Hole Born from a Rotating Star?Authors: Daichi Tsuna, Kazumi Kashiyama, Toshikazu Shigeyama: ABSTRACT: Recently an intriguing transient AT 2018lqh, with only a day-scale duration and a high luminosity of 7×1042 erg s−1, has been discovered. While several possibilities are raised on its origin, the nature of this transient is yet to be unveiled. We propose that a black hole (BH) with ∼30M⊙ forming from a rotating blue supergiant can generate a transient like AT 2018lqh. We find that this scenario can consistently explain the optical/UV emission and the tentative late-time X-ray detection, as well as the radio upper limits. If super-Eddington accretion onto the nascent BH powers the X-ray emission, continued X-ray observations may be able to test the presence of an accretion disk around the

                                        a. CH        b. BH      c. DH       d. FH.

Q16. arXiv:2110.07227 [astro-ph.HE]: [Submitted on 14 Oct 2021]: Long and Short Fast Radio Bursts are Different from Repeating and Non-repeating Transients. Authors : X. J. Li, X. F. Dong, Z. B. Zhang, D. Li: ABSTRACT: We collect 133 Fast Radio Bursts (FRBs), including 110 non-repeating and 23 repeating ones, and systematically investigate their observational properties. To check the frequency dependence of FRB classifications, we define our samples with a central frequency below/above 1GHz as subsample I/II. We find that there is a clear bimodal distribution of pulse width for the subsample I. And If we classify FRBs into short FRBs (\emph{s}FRBs) (<100 ms) and long FRBs (\emph{l}FRBs) (>100 ms) as done for short and long Gamma-Ray Bursts (GRBs), the \emph{s}FRBs at higher central frequency are commonly shorter than those at lower central frequency not only for non-repeating but also repeating \emph{s}FRBs. Secondly, we find that fluence and peak flux density are correlated with a power law relation of F∝S7 p,obs for both \emph{s}FRBs and \emph{l}FRBs whose distributions are obviously different. Thirdly, the \emph{l}FRBs with isotropic energies ranging from 10^42 to 10^44 erg are more energetic than the \emph{s}FRBs in the F−DMEX plane, indicating that they are two representative types. Finally, it is interestingly note that the peak flux density behaves an independence on the redshift when the distance of the FRBs becomes far enough, which is similar to the scenario of peak flux evolving with redshift in the field of GRBs. We predict that fainter FRBs at higher redshift of z>2 can be successfully detected by FAST and SKA in the near 

                       a. instant    b. relation   c. future    d. past.

Q17. arXiv:2110.07864 [astro-ph.IM]:  Fri, 15 Oct 2021 05:35:41 UTC (989 KB)  Submitted on 15 Oct 2021]: CTA sensitivity for probing cosmology and fundamental physics with gamma rays. Authors: Ievgen Vovk, Jonathan Biteau, Humberto Martinez-Huerta, Manuel Meyer, Santiago Pita (for the CTA Consortium): : ABSTRACT: The Cherenkov Telescopic Array (CTA), the next-generation ground-based gamma-ray observatory, will have unprecedented sensitivity, providing answers to open questions in gamma-ray cosmology and fundamental physics. Using simulations of active galactic nuclei observations foreseen in the CTA Key Science Program, we find that CTA will measure gamma-ray absorption on the extragalactic background light with a statistical error below 15% up to the redshift of 2 and detect or establish limits on gamma halos induced by the intergalactic magnetic field of at least 0.3 pG. Extragalactic observations using CTA also demonstrate the potential for testing physics beyond the Standard Model. The best state-of-the-art constraints on the Lorentz invariance violation from astronomical gamma-ray observations will be improved at least two- to threefold. CTA will also probe the parameter space where axion-like particles can represent a significant proportion - if not all - of dark matter. Joint multiwavelength and multimessenger observations, carried out together with other future observatories, will further foster the growth of gamma-ray 

                 a.cosmology    b. detection    c. sensitivity   d. physics.

Q18.  arXiv:2110.07956 [astro-ph.HE]: Fri, 15 Oct 2021 09:20:24 UTC (855 KB)  [Submitted on 15 Oct 2021]: The Hunt for Pevatrons: The Case of Supernova Remnants. by P. Cristofari. :ABSTRACT: The search for Galactic pevatrons is now a well-identified key science project of all instruments operating in the very-high-energy domain. Indeed, in this energy range, the detection of gamma rays clearly indicates that efficient particle acceleration is taking place, and observations can thus help identify which astrophysical sources can energize particles up to the ∼PeV range, thus being pevatrons. In the search for the origin of Galactic cosmic rays (CRs), the PeV range is an important milestone, since the sources of Galactic CRs are expected to accelerate PeV particles. This is how the central scientific goal that is 'solving the mystery of the origin of CRs' has often been distorted into 'finding (a) pevatron(s)'. Since supernova remnants (SNRs) are often cited as the most likely candidates for the origin of CRs, 'finding (a) pevatron(s)' has often become 'confirming that SNRs are pevatrons'. Pleasingly, the first detection(s) of pevatron(s) were not associated to SNRs. Moreover, all clearly detected SNRs have yet revealed to not be pevatrons, and the detection from VHE gamma rays from regions unassociated with SNRs, are reminding us that other astrophysical sites might well be pevatrons. This short review aims at highlighting a few important results on the search for Galactic 

                     a. scintillations    b. tachyons     c. pevatrons      d. SNRs.  

Q19. arXiv:2110.08117 [astro-ph.SR]: Thu, 14 Oct 2021 09:06:17 UTC (1,529 KB): [Submitted on 14 Oct 2021]" Chirality in Astrophysics by Axel Brandenburg. :ABSTRACT: Chirality, or handedness, enters astrophysics in three distinct ways. Magnetic field and vortex lines tend to be helical and have a systematic twist in the northern and southern hemispheres of a star or a galaxy. Helicity is here driven by external factors. Chirality can also enter at the microphysical level and can then be traced back to the parity-breaking weak force. Finally, chirality can arise spontaneously, but this requires not only the presence of an instability, but also the action of nonlinearity. Examples can be found both in magnetohydrodynamics and in astrobiology, where homochirality among biomolecules probably got established at the origin of life. In this review, all three types of chirality production will be explored and 

                            a solicited    b. compared  c. illustrated     d. assesed.

Q20. arXiv:2110.07783 [physics.hist-ph]:  Fri, 15 Oct 2021 00:42:42 UTC (30 KB): [Submitted on 15 Oct 2021]: The Fine-Tuning of the Universe for Life by Luke A. arnes. :ABSTRACT: When a physicist says that a theory is fine-tuned, they mean that it must make a suspiciously precise assumption in order to explain a certain observation. This is evidence that the theory is deficient or incomplete. One particular case of fine-tuning is particularly striking. The data in question are not the precise measurements of cosmology or particle physics, but a more general feature of our universe: it supports the existence of life. This chapter reviews this Fine-Tuning of the Universe for 

                            a. death   b. traffic    c. thought     d. Life.

Q21. arXiv:2110.10175 [astro-ph.GA]: Tue, 19 Oct 2021 18:00:02 UTC (2,690 KB): [Submitted on 19 Oct 2021]: The origins of massive black holes. Authors: Marta Volonteri, Melanie Habouzit, Monica Colpi. : ABSTRACT: Massive black holes (MBHs) inhabit galaxy centers, power luminous quasars and Active Galactic Nuclei (AGN) and shape their cosmic environment with the energy they produce. The origins of MBHs remain a mystery and the recent detection by LIGO/Virgo of an almost 150 solar mass black hole has revitalized the question of whether there is a continuum between ``stellar'' and ``massive'' black holes and what the seeds of MBHs are. Seeds could have formed in the first galaxies, or could be also related to the collapse of horizon-sized regions in the early Universe. Understanding the origins of MBHs straddles fundamental physics, cosmology and astrophysics and it bridges the fields of gravitational wave physics and traditional astronomy. With several facilities in the next 10-15 years we foresee the possibility of discovering MBHs' avenues of formation. In this article we link three main topics: the channels of black hole seed formation, the journey from seeds to massive black holes, the diagnostics on the origins of MBHs. We highlight and critically discuss current unsolved problems and touch on recent developments that stirred the 

                               a. society b. community    c. astronomy    d. cosmology.

Q22. arXiv:2110.10207 [astro-ph.HE]: Tue, 19 Oct 2021 19:03:48 UTC (8,119 KB)[Submitted on 19 Oct 2021]: Radioactive isotopes in the interstellar medium. Roland Diehl:ABSTRACT: Radioactive components of the interstellar medium provide an entirely-different and new aspect to the studies of the interstellar medium. Injected from sources of nucleosynthesis, unstable nuclei decay along their trajectories. Measurements can occur through characteristic gamma rays that are emitted with the decay, or in cosmic material samples through abundances of parent and daughter isotopes as they change with decay. The dynamics and material flows within interstellar medium are thus accessible to measurement, making use of the intrinsic clock that radioactive decay provides. We describe how measurements of radioactive decay have obtained a break-through in studies of the interstellar medium, after first summarizing the characteristics of radioactivity and the sources of unstable 

                             a. decays   b. material    c. trajectories   d. nuclei.

Q23.arXiv:2110.10258 [astro-ph.CO]: Tue, 19 Oct 2021 21:00:21 UTC (3,952 KB)[Submitted on 19 Oct 2021]: Scalar field dark matter with two components: combined approach from particle physics and cosmology. Authors: Eréndira Gutiérrez-Luna, et al.,:ABSTRACT: We explore the possibility of incorporating particle physics motivated scalar fields to the dark matter cosmological model, along with the successful modeling performed by the classical complex scalar field and without spoiling the advantages that this model gives, particularly, the one related to the existence of certain region in the parameter space, which increases the number of neutrino species Neff in the correct amount needed in the early Universe to be consistent with the observed abundance of light elements produced at Big Bang Nucleosynthesis (BBN). We also examine the differences between these models and the priors considered at the edges of the cosmic ladder obtaining that they have a clearly different behavior depending on the combination of the two scalar fields taken into account. In such cases we obtain that depending on the value of the Hubble constant inferred from CMB Planck 2018 data or considering a local value of this constant we can notice a different distribution of matter densities at early or late epochs. We take as a first example, one of the Higgs-like candidates of dark matter and show that if it is added along with the classical complex scalar field, it will give consistent results within the BBN constrain if the heavy scalar field composes less than 58% of the total dark matter. We also use an axion field which has negative self interaction then we will show that (as long as the symmetry breaking scale fa is below the Planck scale) there will be at least a region for which the two-field system is consistent with the constrains. Finally we will explore the possibility of combining the axion and Higgs-like scalar fields and show that there is no set of parameters that allows to be consistent with Neff from BBN constraints. Our results could be relevant on the direct dark matter detection 

                                a. views    b. thoughts    c.programs   d. fields.

Q24. arXiv:2110.10438 [astro-ph.HE]: Wed, 20 Oct 2021 09:05:49 UTC (678 KB)[Submitted on 20 Oct 2021]: Are there magnetars in high-mass X-ray binaries? :Kun Xu, et al., :ABSTRACT: Magnetars form a special population of neutron stars with strong magnetic fields and long spin periods. About 30 magnetars and magnetar candidates known currently are probably isolated. But the possibility that magnetars are in binaries hasn't been excluded. In this work, we perform spin evolution of neutron stars with different magnetic fields in wind-fed high-mass X-ray binaries and compare the spin period distribution with observations, aiming to find magnetars in binaries. Our simulation shows that some of the neutron stars, which have long spin periods or in wide-separation systems, need strong magnetic fields to explain their spin evolution. This implies that there are probably magnetars in high-mass X-ray binaries. Moreover, this can further provide a theoretical basis for some unclear astronomical phenomena, such as the possible origin of periodic fast radio bursts from magnetars in binary 

                                   a. systems      b. stars     c. evolution   d. candidates.

Q25.arXiv:2110.11964 [astro-ph.CO]:  Fri, 22 Oct 2021 18:00:00 UTC (2,587 KB): [Submitted on 22 Oct 2021]: Molecular Chemistry for Dark Matter II: Recombination, Molecule Formation, and Halo MassFunction in Atomic Dark Matter. James Gurian, Donghui Jeong, Michael Ryan, Sarah Shandera: ABSTRACT: Dissipative dark matter predicts rich observable phenomena that can be tested with future large-scale structure surveys. As a specific example, we study atomic dark matter, consisting of a heavy particle and a light particle charged under a dark electromagnetism. In particular, we calculate the cosmological evolution of atomic dark matter focusing on dark recombination and dark-molecule formation. We have obtained the relevant interaction-rate coefficients by re-scaling the rates for normal hydrogen, and evolved the abundances for ionized, atomic, and molecular states using a modified version of RecFAST++. We also provide an analytical approximation for the final abundances. We then calculate the effects of the atomic dark matter on the linear power spectrum, which enter through a dark-photon diffusion and dark acoustic oscillations. At the formation time, the atomic dark matter model suppresses halo abundances on scales smaller than the diffusion scale, just like the warm dark matter models suppress the abundance below the free-streaming scale. The subsequent evolution with radiative cooling, however, will alter the halo mass function further.

                                a.explicitly.   b. scale    c. further     d. warmly.

Q26.arXiv:2110.11975 [astro-ph.CO]:  Fri, 22 Oct 2021 18:00:03 UTC (604 KB)[Submitted on 22 Oct 2021]: Background of radio photons from primordial black holes. Shikhar Mittal (TIFR), Girish Kulkarni (TIFR): ABSTRACT: We compute the isotropic radiation background due to Hawking emission from primordial black holes (PBHs), and examine if this background is a viable option in explaining the excess radiowave background observed by the ARCADE2 and LWA1 experiments at ≲1GHz. We find that even under the extreme assumption that all of the dark matter is in the form of PBHs, the radio brightness temperature induced by Hawking evaporation of PBHs is O(10−46)K, highly subdominant compared to the cosmic microwave background. The main reason for this is that for PBHs in the mass range ∼1012-1014kg, which can be constrained by Hawking emission, the spectrum peaks at 107 to 105eV. As the Hawking spectrum is power law suppressed towards lower energies, negligible flux of μeV photons is obtained. The peak of the Hawking spectrum shifts to lower energies for higher masses, but the number density is low and so is the specific intensity. Because Hawking emission from PBHs is thus unable to explain the observed excess radio background, we also consider the alternative possibility of radio emission from gas accretion onto supermassive PBHs. These PBHs can readily produce strong radio emission that could easily explain the ARCADE2/LWA1 

                               a. emission   b. excess   c. density      d. reason.

Q27. arXiv:2110.11982 [astro-ph.SR]: Fri, 22 Oct 2021 18:05:44 UTC (1,001 KB): [Submitted on 22 Oct 2021]: New constraints on the minimum mass for thermonuclear lithium burning in brown dwarfs. Eduardo L. Martín, Nicolas Lodieu, Carlos del Burgo. :ABSTRACT: The theory of substellar evolution predicts that there is a sharp mass boundary between lithium and non-lithium brown dwarfs, not far below the substellar-mass limit. The imprint of thermonuclear burning is carved on the surface lithium abundance of substellar-mass objects during the first few hundred million years of their evolution, leading to a sharp boundary between lithium and non-lithium brown dwarfs, so-called, the lithium test. New optical spectroscopic observations of the binaries DENIS+J063001.4-184014 and DENIS+J225210.7-173013 obtained using the 10.4-m Gran Telescopio de Canarias are reported here. They allow us to re-determine their combined optical spectral types (M9.5 and L6.5, respectively) and to search for the presence of the LiI resonance doublet. The non detection of the LiI feature in the combined spectrum of DENIS\,J063001.4−184014AB is converted into estimates for the depletion of lithium in the individual components of this binary system. In DENIS\,J225210.7−173013AB we report the detection of a weak LiI feature which we tentatively ascribe as arising from the contribution of the T3.5-type secondary. Combining our results with data for seven other brown dwarf binaries in the literature treated in a self-consistent way, we confirm that there is indeed a sharp transition in mass for lithium depletion in brown dwarfs, as expected from theoretical calculations. We estimate such mass boundary is observationally located at 51.48/+0.22/−4.00 MJup, which is lower than the theoretical                                               

             a. predictions   b. calculations   c. features    d. determinations.

Q28.arXiv:2110.13053 [astro-ph.SR]:Mon, 25 Oct 2021 15:45:42 UTC (3,194 KB): [Submitted on 25 Oct 2021]: Near-infrared studies of nova V1674 Herculis: A shocking record-breaker. C. E. Woodward, D. P. K. Banerjee, T. R. Geballe, K. L. Page, S. Starrfield, R. M. Wagner: ABSTRACT: We present near infrared spectroscopy of Nova Herculis 2021 (V1674 Her), obtained over the first 70 days of its evolution. This fastest nova on record displays a rich emission line spectrum, including strong coronal line emission with complex structures. The hydrogen line fluxes, combined with a distance of 4.7 (+1.3 / -1.0) kpc, give an upper limit to the hydrogen ejected mass of 1.4 (+0.8 / -1.2) 10^{-3} solar masses. The coronal lines appeared at day 11.5, the earliest onset yet observed for any classical nova, before there was an obvious source of ionizing radiation. We argue that the gas cannot be photoionized, at least in the earliest phase, and must be shocked. Its temperature is estimated to be 10^{5.57 +/- 0.05} K on day 11.5. Tentative analysis indicates a solar abundance of aluminum and an underabundance of calcium, relative to silicon, with respect to solar values in the ejecta. Further, we show that the vexing problem of whether collisional or photoionization is responsible for coronal emission in classical novae can be resolved by correlating the temporal sequence in which the X-ray supersoft phase and the near-infrared coronal line emission

                             a appear.    b. destroyed    c. enhanced   d. determinantal.

Q29. arXiv:2111.02611 [astro-ph.HE]: Thu, 4 Nov 2021 03:42:04 UTC (133 KB):[Submitted on 4 Nov 2021]: The Origin of High Energy Emission in the Young Radio Source PKS 1718-649. Authors: Małgosia Sobolewska, et al., :ABSTRACT: We present a model for the broadband radio-to-γ-ray spectral energy distribution of the compact radio source, PKS 1718-649. Because of its young age (100 years) and proximity (z=0.014), PKS 1718-649 offers a unique opportunity to study nuclear conditions and the jet/host galaxy feedback process at the time of an initial radio jet expansion. PKS 1718-649 is one of a handful of young radio jets with γ-ray emission confirmed with the Fermi/LAT detector. We show that this γ-ray emission can be successfully explained by Inverse Compton scattering of the ultraviolet photons, presumably from an accretion flow, off non-thermal electrons in the expanding radio lobes. The origin of the X-ray emission in PKS 1718-649 is more elusive. While Inverse Compton scattering of the infrared photons emitted by a cold gas in the vicinity of the expanding radio lobes contributes significantly to the X-ray band, the data require that an additional X-ray emission mechanism is at work, e.g. a weak X-ray corona or a radiatively inefficient accretion flow, expected from a LINER type nucleus such as that of PKS 1718-649. We find that the jet in PKS 1718-649 has low power, Lj≃2.2×10^42 erg s^−1, and expands in an environment with density n0≃20 cm^−3. The inferred mass accretion rate and gas mass reservoir within 50-100 pc are consistent with estimates from the literature obtained by tracing molecular gas in the innermost region of the host galaxy with SINFONI and 

                                      a. sin     b. cold     c. ALMA   d. hotair.

Q30. arXiv:2111.09657 [astro-ph.GA]: Thu, 18 Nov 2021 12:27:43 UTC (603 KB): [Submitted on 18 Nov 2021]: Probing the shape of the Milky Way dark matter halo with hypervelocity stars: a new method. Arianna Gallo, Luisa Ostorero, Sankha Subhra Chakrabarty, Stefano Ebagezio, Antonaldo Diaferio.: ABSTRACT: We propose a new method to determine the shape of the gravitational potential of the dark matter (DM) halo of the Milky Way (MW) with the galactocentric tangential velocities of a sample of hypervelocity stars (HVSs). We compute the trajectories of different samples of HVSs in a MW where the baryon distribution is axisymmetric and the DM potential either is spherical or is spheroidal or triaxial with radial-dependent axis ratios. We determine the shape of the DM potential with the distribution of the latitudinal velocity |vϑ| in axisymmetric Galactic potentials, or with the distribution of |vϑ | and of a function v¯φ of the azimuthal velocity in non-axisymmetric Galactic potentials. We recover the correct shape of the DM potential by comparing the distribution of |vϑ| and v¯φ against the corresponding distributions of mock samples of HVSs that traveled in DM halos of different shapes. We use the largest possible sample of ∼800 HVSs of 4 M⊙ ejected with the Hills mechanism at a rate ∼10^−4 yr^−1, currently outgoing, and located at more than 10 kpc from the Galactic center. In the ideal case of galactocentric velocities with null uncertainties, our method recovers the correct shape of the DM potential with a success rate S≳89% in axisymmetric Galactic potentials, and S>96% in the explored non-axisymmetric cases. The unsuccessful cases yield axis ratios of the DM potential that are off by ±0.1. The success rate decreases with decreasing sample size: for ∼80 HVSs, close to the current number of HVS candidates, S is in the range ∼40%−60%, depending on the actual shape of the DM halo. A robust determination of the shape of the DM potential thus requires increasing by a factor ∼10 the size of the sample of genuine HVSs with measured galactocentric 

                          a. velocity    b. recovery    c. shape   d. ejection.

Q31. arXiv:2111.09720 [astro-ph.GA]: Thu, 18 Nov 2021 14:27:52 UTC (7,765 KB): [Submitted on 18 Nov 2021]: The formation and early evolution of embedded star clusters in spiral galaxies. Steven Rieder, Clare Dobbs, Thomas Bending, Kong You Liow, James Wurster, : ABSTRACT: We present Ekster, a new method for simulating star clusters from birth in a live galaxy simulation that combines the smoothed-particle hydrodynamics (SPH) method Phantom with the N-body method PeTar. With Ekster, it becomes possible to simulate individual stars in a simulation with only moderately high resolution for the gas, allowing us to study whole sections of a galaxy rather than be restricted to individual clouds. We use this method to simulate star and star cluster formation in spiral arms, investigating massive GMCs and spiral arm regions with lower mass clouds, from two galaxy models with different spiral potentials. After selecting these regions from pre-run galaxy simulations, we re-sample the particles to obtain a higher resolution. We then re-simulate these regions for 3 Myr to study where and how star clusters form. We analyse the early evolution of the embedded star clusters in these regions. We find that the massive GMC regions, which are more common with stronger spiral arms, form more massive clusters than the sections of spiral arms containing lower mass clouds. Clusters form both by accreting gas and by merging with other proto-clusters, the latter happening more frequently in the denser GMC 

                                     a.  clouds   b. regions    c. formation     d. evolution.

Q32. arXiv:2111.09865 [astro-ph.GA]: Thu, 18 Nov 2021 18:45:42 UTC (13,211 KB): [Submitted on 18 Nov 2021]: The Hosts of X-ray Absorption Lines Toward AGNs. Maggie C. Huber, Joel N. Bregman. :ABSTRACT: Most baryonic matter in the universe exists in gaseous form and can be found in structures such as galactic halos and the low-density intergalactic medium. proposed-ray spectroscopy missions such as Athena, Arcus, and Lynx will have the capability to identify absorption lines in spectra toward bright active galactic nuclei (AGNs), which can be used as a tool to probe this missing matter. In this study, we examine the optical fields surrounding 15 primary observing targets and identify the foreground galaxies and galaxy groups that are potential hosts of absorption. We record the basic properties of the potential host and their angular and physical separation from the AGN line of sight. This process is done by marking the location of various galaxies and groups in optical images of the field surrounding the target and plotting their angular separation vs. redshift to gauge physical proximity to the background source. We identify the surrounding objects according to those which have measured redshifts and those that require 

                                       a. halos   b. lines   c. locations    d. them.

Q33. arXiv:2111.09795 [math.AP]:Thu, 18 Nov 2021 16:53:48 UTC (905 KB):[Submitted on 18 Nov 2021]: Time reversal of surface plasmons. Olivier Pinaud. :ABSTRACT: We study in this work the so-called "instantaneous time mirrors" in the context of surface plasmons. The latter are associated with high frequency waves at the surface of a conducting sheet. Instantaneous time mirrors were introduced by M. Fink et al, with the idea that singular perturbations in the time variable in a wave-type equation create a time-reversed focusing wave. We consider the time-dependent three-dimensional Maxwell's equations, coupled to Drude's model for the description of the surface current. The time mirror is modeled by a sudden, strong, change in the Drude weight of the electrons on the sheet. Our goal is to characterize the time-reversed wave, in particular to quantify the quality of refocusing. We establish that the latter depends on the distance of the source to the sheet, and on some physical parameters such as the relaxation time of the electrons. We also show that, in addition to the plasmonic wave, the time mirror generates a free propagating wave that offers, contrary to the surface wave, some resolution in the direction orthogonal to the sheet. Blurring effects due to non-instantaneous mirrors are finally 

                               a. researched   b. investigated  c. modeled    d. created.

Q34. arXiv:2111.10384 [astro-ph.GA]:Fri, 19 Nov 2021 19:00:01 UTC (2,793 KB):[Submitted on 19 Nov 2021]: How are Red and Blue Quasars Different? The Radio Properties. V. A. Fawcett, D. M. Alexander, D. J. Rosario, L. Klindt.: ABSTRACT: A non-negligible fraction of quasars are red at optical wavelengths, indicating (in the majority of cases) that the accretion disc is obscured by a column of dust which extinguishes the shorter-wavelength blue emission. In this paper, we summarize recent work by our group, where we find fundamental differences in the radio properties of SDSS optically-selected red quasars. We also present new analyses, using a consistent color-selected quasar parent sample matched to four radio surveys (FIRST, VLA Stripe 82, VLA COSMOS 3 GHz, and LoTSS DR1) across a frequency range 144 MHz-3 GHz and four orders of magnitude in radio flux. We show that red quasars have enhanced small-scale radio emission (~kpc) that peaks around the radio-quiet threshold (defined as the ratio of 1.4 GHz luminosity to 6 micron luminosity) across the four radio samples. Exploring the potential mechanisms behind this enhancement, we rule out star-formation and propose either small-scale synchrotron jets, frustrated jets, or dusty winds interacting with the interstellar medium; the latter two scenarios would provide a more direct connection between opacity (dust; gas) and the production of the radio emission. In our future study, using new multi-band uGMRT data, we aim to robustly distinguish between these 

                                 a. samples  b. jets    c. mechanisms   d. scenarios

Q35.  arXiv:2111.10615 [astro-ph.HE]: Sat, 20 Nov 2021 15:43:38 UTC (609 KB): [Submitted on 20 Nov 2021]: Pulsar Polarization Arrays: by Tao Liu, Xuzixiang Lou, Jing Ren: ABSTRACT: Pulsar timing arrays (PTAs) consisting of widely distributed and well-timed millisecond pulsars can serve as a galactic interferometer to measure gravitational waves. With the same data acquired for PTAs, we propose to develop pulsar polarization arrays (PPAs), to explore astrophysics and fundamental physics. As in the case of PTAs, PPAs are best suited to reveal temporal and spatial correlations at large scales that are hard to mimic by local noise. To demonstrate the physical potential of PPAs, we consider detection of ultralight axion-like dark matter (ALDM), through cosmic birefringence induced by its Chern-Simon coupling. Because of its tiny mass, the ultralight ALDM can be generated as a Bose-Einstein condensate, characterized by a strong wavy nature. Incorporating both temporal and spatial correlations of the signal, we show that PPAs have a potential to probe the Chern-Simon coupling up to ∼10^−14−10^−17GeV^−1, with a mass range 

 a.∼10^−27−10^−21eV b.∼10^−28−10^−21eV c.∼10^−29−10^−21eV  and                     d.∼10^−30−10^−21eV.

Q36. arXiv:2111.10870 [astro-ph.HE]: Sun, 21 Nov 2021 18:13:39 UTC (860 KB):[Submitted on 21 Nov 2021]: Quantum synchro-curvature masers and their application to neutron stars. Hiroko Tomoda, Tomoya Naoe, Shoichi Yamada. : ABSTRACT:  We explore the possibility of synchro-curvature maser in the magnetosphere of neutron stars (NSs). Unlike previous studies, we employ relativistic quantum mechanics, solving the Dirac equation for an electron in helical magnetic fields and calculating the radiative transition rates perturbatively. Assuming that the curvature of magnetic-field lines is much larger than the Larmor radius, we utilize adiabatic spinor rotations to obtain the wave functions of an electron. We classify the electron states further either by the spin operator projected on the magnetic field or by the helicity operator. We then evaluate numerically the true absorption rates accounting for the induced emission for some parameter values typical to the outer gaps of different types of NSs. We show that maser is indeed possible for a range of parameters. We will also present the dependence on those parameters systematically. We finally give a crude estimate of the amplification factor in the outer gap of NSs, which seems to favor millisecond pulsars as the host of maser 

                           a. mechanics     b. relativity    c. emissions    d. parameters.

Q37. arXiv:2111.11012 [physics.plasm-ph]:   Mon, 22 Nov 2021 06:32:40 UTC (1,062 KB): [Submitted on 22 Nov 2021]: Brilliant circularly polarized γ-ray sources via single-shot laser plasma interaction. Yu Wang, Mamutjan Ababekri, Feng Wan, Qian Zhao, Chong Lv, Xue-Guang Ren, Zhong-Feng Xu, Yong-Tao Zhao, Jian-Xing Li. :ABSTRACT: Circularly polarized (CP) γ-ray sources are versatile for broad applications in nuclear physics, high-energy physics and astrophysics. The laser-plasma based particle accelerators provide accessibility for much higher flux γ-ray sources than conventional approaches, in which, however, the circular polarization properties of emitted γ-photons are used to be neglected. In this letter, we show that brilliant CP γ-ray beams can be generated via the combination of laser plasma wakefield acceleration and plasma mirror techniques. In weakly nonlinear Compton scattering scheme with moderate laser intensities, the helicity of the driving laser can be transferred to the emitted γ-photons, and their average polarization degree can reach about ∼37% (21%) with a peak brilliance of ≳1021 photons/(s ⋅ mm2⋅ mrad2⋅ 0.1% BW) around 1~MeV (100~MeV). Moreover, our proposed method is easily feasible and robust with respect to the laser and plasma 

                         a. properties .b. parameters. c. excitons  d. applications.

Q38.arXiv:2111.11033 [physics.geo-ph]: Mon, 22 Nov 2021 07:39:42 UTC (991 KB): [Submitted on 22 Nov 2021]: Oxygen-driven enhancement of electron correlation in hexagonal iron at Earth's inner core conditions. Bo Gyu Jang, Yu He, Ji Hoon Shim, Ho-kwang Mao, Duck Young Kim. :ABSTRACT: Earth's inner core consists of mainly iron with a bit of light elements. Understanding of its structure and related physical properties has been elusive for both experiment and theory due to its required extremely high pressure and temperature conditions. Here, using density functional theory plus dynamical mean field theory, we demonstrate that oxygen atoms energetically stabilize hexagonal structured iron at the inner core condition. Electrical resistivity is much enhanced compared with pure hcp-Fe, supporting the conventional thermal convection model. Moreover, our calculated seismic velocity shows a quantitative match with geologically observed Preliminary Reference Earth Model

                         a. data   b. constants   c. parameters   d. experiments.

Q39.arXiv:2112.01546 [astro-ph.GA]: Thu, 2 Dec 2021 19:00:02 UTC (1,802 KB): [Submitted on 2 Dec 2021]: Neutral Gas within 20,000 Schwarzschild radii of Sagittarius A*: Authors: Elena M. Murchikova, Tianshu Wang, Brian Mason, Roger D. Blandford.  :ABSTRACT: Murchikova et al 2019 discovered a disk of cool ionized gas within 20,000 Schwarzschild radii of the Milky Way's Galactic Center black hole Sagittarius A*. They further demonstrated that the ionizing photon flux in the region is enough to keep the disk ionized, but there is not ample excess of this radiation. This raised the possibility that some neutral gas could also be in the region shielded within the cool ionized clumps. Here we present ALMA observations of a broad 1.3 millimeter hydrogen recombination line H30alpha: n = 31 -> 30, conducted during the flyby of the S0-2 star by Sgr A*. We report that the velocity-integrated H30alpha line flux two month prior to the S0-2 pericenter passage is about 20% larger than it was one month prior to the passage. The S0-2 is a strong source of ionizing radiation moving at several thousand kilometers per second during the approach. Such a source is capable of ionising parcels of neural gas along its trajectory, resulting in variation of the recombination line spectra from epoch to epoch. We conclude that there are at least (6.6 +- 3.3) x 10^{-6} Msun of neutral gas within 20,000 Schwarzschild radii of 

                                      a. Cgr A*     b. bgr A*   c. Sgr A*    d. Bgr A*.

Q40.arXiv:2112.01748 [astro-ph.HE]: Fri, 3 Dec 2021 07:06:58 UTC (1,427 KB): [Submitted on 3 Dec 2021]: Could TDE outflows produce the PeV neutrino events? Authors: Han-Ji Wu, Guo-Bin Mou, Kai Wang, Wei Wang, Zhuo Li.  ABSTRACT: The origin of ultra-high energy neutrinos still lacks observational evidence, besides, the physical mechanism is also unclear. There is an association of a PeV neutrino event (IceCube-191001A) with an optical tidal disruption event (TDE, AT2019dsg) which was detected 6 months ahead from IceCube-191001A. The numerical simulations and observations suggested that a TDE can produce ultrafast outflows, which will interact with clouds near the supermassive black hole. In this paper, we study the interactions between TDE outflows and clouds and the possible production. In the shock waves generated by the outflow-cloud interactions, protons can be accelerated to ∼ 60 PeV with the outflow velocity 0.07 c and kinetic luminosity 1045erg/s. PeV neutrinos can be produced through hadronic reactions. The calculation illustrates that the expected PeV neutrino event from AT2019dsg is 0.014 for a power-law proton energy distribution of Γ=1.5 and 0.0016 for Γ=1.9. The GeV --TeV γ-rays through hadronic processes are lower than the present observed limits. Outflows escaped from the TDE center colliding with clouds, which also can naturally explain the half-year delay between the neutrino event and

                                                   a. SDE     b. TDE   c. JDE   GDE.

Q41. arXiv:2112.01737 [physics.ins-det]: Fri, 3 Dec 2021 06:30:15 UTC (246 KB): [Submitted on 3 Dec 2021]: Neutral bremsstrahlung electroluminescence in noble liquids. Authors: E. Borisova, A. Buzulutskov. :ABSTRACT:  Proportional electroluminescence (EL) is the physical effect used in two-phase dark matter detectors, to optically record in the gas phase the ionization signal produced by particle scattering in the liquid phase. In our previous works the presence of a new EL mechanism in noble gases, namely that of neutral bremsstrahlung (NBrS), was demonstrated both theoretically and experimentally, in addition to the ordinary EL mechanism due to excimer emission. In this work we show that the similar theoretical approach can apply to noble liquids, namely to liquid helium, neon, argon, krypton and xenon. In particular, the photon yields and spectra for NBrS EL in noble liquids have for the first time been calculated, using the electron energy and transport parameters obtained in the framework of Cohen-Lekner and Atrazhev theory. The relevance of the results obtained to the development of noble liquid detectors for dark matter searches and neutrino experiments is 

                             a. elaborated   b. ventured   c. specified   d. discussed.

Q42. arXiv:2112.03959 [astro-ph.SR]: Tue, 7 Dec 2021 19:30:07 UTC (1,773 KB): [Submitted on 7 Dec 2021]: An eccentric Brown Dwarf eclipsing an M dwarf. ABSTRACT: Caleb I. Cañas, et al., :ABSTRACT: We report the discovery of a M=67±2MJ brown dwarf transiting the early M dwarf TOI-2119 on an eccentric orbit (e=0.3362±0.0005) at an orbital period of 7.200861±0.000005 days. We confirm the brown dwarf nature of the transiting companion using a combination of ground-based and space-based photometry and high-precision velocimetry from the Habitable-zone Planet Finder. Detection of the secondary eclipse with TESS photometry enables a precise determination of the eccentricity and reveals the brown dwarf has a brightness temperature of 2100±80 K, a value which is consistent with an early L dwarf. TOI-2119 is one of the most eccentric known brown dwarfs with P<10 days, possibly due to the long circularization timescales for an object orbiting an M dwarf. We assess the prospects for determining the obliquity of the host star to probe formation scenarios and the possibility of additional companions in the system using Gaia EDR3 and our radial

                    a.  gammas  b. velocities c. angular momentum  d. temperatures.

Q43. arXiv:2112.04003 [physics.optics]: Tue, 7 Dec 2021 21:33:19 UTC (1,272 KB):

[Submitted on 7 Dec 2021]: Refraction of space-time wave packets in a dispersive

medium. Authors, Murat Yessenov, Sanaz Faryadras, Sepehr Benis, David J. Hagan,

Eric W. Van Stryland, Ayman F. Abouraddy: :ABSTRACT: Space-time (ST) wave packets

are a class of pulsed optical beams whose spatio-temporal spectral structure results

in propagation invariance, tunable group velocity, and fascinating refractive

phenomena. Here, we investigate the refraction of ST wave packets at a planar

interface between two dispersive, homogeneous, isotropic media. We formulate a

new refractive invariant for ST wave packets in this configuration, from which

we obtain a law of refraction that determines the change in their group velocity

across the interface. We verify this new refraction law in ZnSe and CdSe, both of

which manifest large chromatic dispersion at near-infrared frequencies in the vicinity

of their band edges. ST wave packets can thus be a tool in nonlinear optics for

bridging large group-velocity mismatches in highly dispersive a. sceans b. scenarios c. spectra d. refractions.

Q44.arXiv:2112.04272 [physics.plasm-ph]: Wed, 8 Dec 2021 13:06:49 UTC (493 KB):

[Submitted on 8 Dec 2021]: Overstability of Plasma Slow Electron Holes. Author:

I H Hutchinson. :ABSTRACT: Sufficient conditions are found on the ion velocity

distribution fi and potential amplitude for stability of steady electron holes moving

at slow speeds, coinciding with the bulk of fi. Fully establishing stability requires

calculation of the ion response to shift potential perturbations having an entire

range of oscillatory frequencies, because under some conditions real frequencies

intermediate between the ion and electron responses prove to be unstable even

when the extremes are not. The mechanism of this overstability is explained and

calculated in detail. Electron holes of peak potential ψ less than approximately

0.01 times the background temperature (ψ≲0.01T0/e) avoid the oscillatory instability

entirely. For them, the \emph{necessary} condition that there be a local minimum in

fi in which the hole resides is also \emph{sufficient}, unless the magnetic field B is

low enough to permit the transverse instability having finite wavenumber k

perpendicular to a. B b. C c. D d. E.

Q45. arXiv:2112.05835 [astro-ph.SR]: Fri, 10 Dec 2021 21:17:14 UTC (1,547 KB)[Submitted on 10 Dec 2021]: Ground-based observations of the ZZ Ceti star HS 1625+1231. Csilla Kalup, Zsófia Bognár, Ádám Sódor. :ABSTRACT: We present the results of our detailed light curve analysis of the ZZ Ceti star HS 1625+1231. We collected photometric time series data at Konkoly Observatory on 14 nights, and performed Fourier analysis of these data sets. We detected 11 significant frequencies, where six of them are found to be independent pulsation modes in the 514 - 881 s period range. By utilising these frequencies, we performed preliminary asteroseismic investigations to give constraints on the main physical parameters, and to derive seismic distances for the star. Finally, we compared the astrometric distance provided by the Gaia EDR3 data with those seismic distances. Our selected model, considering both the spectroscopic measurements and the distance value provided by Gaia, has Teff = 11 000 K and M∗ = 

                           a.  1.0  M⊙     b.   2.0 M⊙    c. 0.60  M⊙     d.  0.80 M⊙.

Q46.arXiv:2112.05952 [astro-ph.HE]: Sat, 11 Dec 2021 11:06:35 UTC (600 KB)[Submitted on 11 Dec 2021]: Cosmology with Very-High-Energy Gamma Rays. Authors: Elisa Pueschel, Jonathan Biteau. :ABSTRACT: In this chapter, we discuss the contributions of gamma-ray astronomy at TeV energies to our understanding of the visible content and structure of the universe. We start from the present epoch with the second most intense electromagnetic background field after the CMB: the extragalactic background light (EBL). The EBL is composed of all the light emitted by stars and galaxies since the beginning of reionization, including light absorbed and re-emitted by dust. As such, the EBL traces the history of radiating matter in the universe. We then further dive into the large voids of the universe to study the large-scale magnetic fields that should permeate them. These fields could originate from the onset of structure formation or early phase transitions, bringing us back to the infancy of the universe. We conclude by looking back to the elusive Planck time scale, where the standard models of cosmology and particle physics are no longer applicable. Observations with current-generation gamma-ray astronomy experiments have now started to scratch the surface of 

                                  a. Gamma Rays  b. energies   c. field     d. cosmology.

Q47.  arXiv:2112.06076 [astro-ph.SR]: Sat, 11 Dec 2021 21:39:56 UTC (154 KB): [Submitted on 11 Dec 2021]: The curious case of Betelgeuse. by Jacco Th. van Loon.  : ABSTRACT: Betelgeuse is the nearest red supergiant, one of the brightest stars in our sky, and statistically speaking it would be expected to be "typical". Yet it exhibits many features that seem "curious", to say the least. For instance it has a high proper motion. It rotates fast. It has little dust. It dimmed unexpectedly. Is any of these, and other, phenomena atypical, and taken together does it make Betelgeuse atypical? This is important to know, because we need to know whether Betelgeuse might be a prototype of red supergiants in general, or certain subclasses of red supergiants, since we can study it in such great detail. It is also important to know as it may be a link to understanding other, apparently atypical cases such as supernova 1987A, and maybe even such exotica as Thorne-Żytkov objects. Studying this question in itself helps us understand how we deal with rarity and coincidence in understanding the Universe we live 

                   a. in      b. outward   c. factually      d. accicidentally. 

Q48. arXiv:2112.06232 [astro-ph.HE]: Sun, 12 Dec 2021 13:24:15 UTC (3,941 KB): [Submitted on 12 Dec 2021]: Astrophysical Neutrinos and Blazars. Paolo Giommi, Paolo Padovani: ABSTRACT: We review and discuss recent results on the search for correlations between astrophysical neutrinos and gamma-ray-detected sources, with many extra-galactic studies reporting potential associations with different types of blazars. We investigate possible dependencies on blazar sub-classes by using the largest catalogues and all the multi-frequency data available. Through the study of similarities and differences in these sources we conclude that blazars come in two distinct flavors: LBLs and IHBLs (low-energy-peaked and intermediate-high-energy-peaked objects). These are distinguished by widely different properties such as the overall spectral energy distribution shape, jet speed, cosmological evolution, broad-band spectral variability, and optical polarization properties. Although blazars of all types have been proposed as neutrino sources, evidence is accumulating in favor of IHBLs being the counterparts of astrophysical neutrinos. If this is indeed the case, we argue that the peculiar observational properties of IHBLs may be indirectly related to proton acceleration to very high 

                                  a. variability   b. energies    c. velocities    d. flavors.

Q49.arXiv:2112.06971 [astro-ph.GA]: Mon, 13 Dec 2021 19:13:08 UTC (21,397 KB): [Submitted on 13 Dec 2021]: Reading M87's DNA: A Double Helix revealing a large scale Helical Magnetic Field. Authors: Alice Pasetto, Carlos Carrasco-Gonzalez, Jose L. Gomez, Jose M. Marti, Manel Perucho, Shane P. O'Sullivan, Craig Anderson, Daniel Jacobo Diaz-Gonzalez, Antonio Fuentes, John Wardle: ABSTRACT: We present unprecedented high fidelity radio images of the M87 jet. We analyzed Jansky Very Large Array (VLA) broadband, full polarization, radio data from 4 to 18 GHz. The observations were taken with the most extended configuration (A configuration), which allow the study of the emission of the jet up to kpc scales with a linear resolution ∼10 pc. The high sensitivity and resolution of our data allow to resolve the jet width. We confirm a double-helix morphology of the jet material between ∼300 pc and ∼1 kpc. We found a gradient of the polarization degree with a minimum at the projected axis and maxima at the jet edges, and a gradient in the Faraday depth with opposite signs at the jet edges. We also found that the behavior of the polarization properties along the wide range of frequencies is consistent with internal Faraday depolarization. All these characteristics strongly support the presence of a helical magnetic field in the M87 jet up to 1 kpc from the central black hole although the jet is most likely particle dominated at these large scales. Therefore, we propose a plausible scenario in which the helical configuration of the magnetic field has been maintained to large scales thanks to the presence of Kelvin-Helmholtz 

                                 a. criteria    b. degrees   c. joints   d. instabilities.

Q50. arXiv:2112.06930 [hep-ph]: Mon, 13 Dec 2021 19:00:00 UTC (540 KB): [Submitted on 13 Dec 2021]: The ups and downs of inelastic dark matter: Electron recoils from terrestrial upscattering. Authors: Timon Emken, Jonas Frerick, Saniya Heeba, Felix Kahlhoefer. :ABSTRACT:The growing interest in the interactions between dark matter particles and electrons has received a further boost by the observation of an excess in electron recoil events in the XENON1T experiment. Of particular interest are dark matter models in which the scattering process is inelastic, such that the ground state can upscatter into an excited state. The subsequent exothermic downscattering of such excited states on electrons can lead to observable signals in direct detection experiments and gives a good fit to the XENON1T excess. In this work, we study terrestrial upscattering, i.e. inelastic scattering of dark matter particles on nuclei in the Earth, as a plausible origin of such excited states. Using both analytical and Monte Carlo methods, we obtain detailed predictions of their density and velocity distribution. These results enable us to explore the time dependence of the flux of excited states resulting from the rotation of the Earth. For the case of XENON1T, we find the resulting daily modulation of the electron recoil signal to be at the level of 10% with a strong dependence on the dark matter

                                      a. energy    b. mass  c. state     d. properties.

Q51. arXiv:2112.07778 [astro-ph.GA]: Tue, 14 Dec 2021 22:57:09 UTC (7,298 KB): [Submitted on 14 Dec 2021]: The dark mass signature in the orbit of S2: Gernot Heißel, Thibaut Paumard, Guy Perrin, Frédéric Vincent. ABSTRACT: Aims. We explore a strategy for how the Schwarzschild and mass precessions can be separated from each other despite their secular interference, by pinpointing their signatures within a single orbit. From these insights, we then seek to assess the prospects for improving the dark mass constraints in the coming years. Methods. We analysed the dependence of the osculating orbital elements and of the observables on true anomaly, and we compared these functions for models with and without extended mass. We then translated the maximum astrometric impacts within one orbit to detection thresholds given hypothetical data of different accuracies. These theoretical investigations were then supported and complemented by an extensive mock-data fitting analysis. Results. We have four main results. 1. While the mass precession almost exclusively impacts the orbit in the apocentre half, the Schwarzschild precession almost exclusively impacts it in the pericentre half, allowing for a clear separation of the effects. 2. Data that are limited to the pericentre half are not sensitive to a dark mass, while data limited to the apocentre half are, but only to a limited extent. 3. A full orbit of data is required to substantially constrain a dark mass. 4. For a full orbit of astrometric and spectroscopic data, the astrometric component in the pericentre half plays the stronger role in constraining the dark mass than the astrometric data in the apocentre half. Furthermore, we determine the 1{\sigma} dark mass detection thresholds given different datasets on one full orbit. In particular, with a full orbit of data of 50 microarcseconds (VLTI/GRAVITY) and 10 km/s (VLT/SINFONI) precision, the 1{\sigma} bound would improve to about 1000 solar masses, for

                            a. scenario   b. version     c. example. d. illustration 

Q52..arXiv:2112.10964 [astro-ph.HE]: Tue, 21 Dec 2021 03:39:53 UTC (1,438 KB): [Submitted on 21 Dec 2021]: On the Radiation Fields of Fast Radio Bursts Close to Sources. Yu Zhang, Hui-Chun Wu. ABSTRACT: Fast radio bursts (FRBs) are coherent powerful radio transients with cosmological origins. The detected galactic FRB reveals that magnetars can generate FRBs, however the mechanism still remains enigmatic. Characteristics of FRBs are limited to observable quantities such as luminosity, duration, spectrum and repetition etc. Due to the uncertainties of triggering mechanisms and source sites within or out of magnetospheres of neutron stars, status of FRBs close to their sources are unknown. As an extreme astronomical event, FRBs could accompany with energy-comparable or even more powerful x/-ray counterparts. Here, we study the interaction of ultrastrong radio pulses in GHz and high-energy photons in GeV. Particle-in-cell simulations show that at the field-strength of about 3*10^12V/cm, quantum cascade effects can generate dense pair plasmas and the radio pulses are significantly depleted. Therefore, GHz radio pulses of stronger than 3*10^12V/cm is difficult to escape from emitters if accompanying with GeV photons. This process could afford a limit to the FRB field strength nearby sources. Investigation on the toleration of >10^12V/cm radio waves for potential plasma/beam emitters in neutron-star scenerios should be helpful to distinguish the precise mechanism of 

                           a  FRBs       b. Neutron stars    c. radio pulses    d. sources.  

Q53.arXiv:2112.11169 [hep-th]: Tue, 21 Dec 2021 13:05:33 UTC (210 KB): [Submitted on 21 Dec 2021]: On models of Cosmology. Poula Tadros, Mohamed Assaad Abdel-Raouf. : ABSTRACT:In this work the most promising string cosmology models are re-viewed model by model in detail. These models are based on conceptsform string theory and heterotic M theory to construct possible scenar-ios for the beginning and the evolution of the universe. In all models asin standard cosmology the problem of particle-antiparticle asymmetryarises, the issue is that all models predict equal number of matter andantimatter to be present in the universe, this contradicts the observa-tions that the number of antiparticle is much less than the number ofparticles. In order to solve the asymmetry dilemma of particles andantiparticles, it is proposed that particles and antiparticles were dis-tributed in the brane and antibrane, respectively, immediately afterthe collision. Implications of these scenarios are discussed in

                         a. elaboration    b. explicitly     c. detail      d. short.

Q54. arXiv:2112.11401 [hep-th]: Tue, 21 Dec 2021 18:04:20 UTC (27 KB):[Submitted on 21 Dec 2021]: Double Quantization. Authors. Giulia Gubitosi, Fedele Lizzi, José Javier Relancio, Patrizia Vitale.    :ABSTRACT: In a quantum gravity theory, it is expected that the classical notion of spacetime disappears, leading to a quantum structure with new properties. A possible way to take into account these quantum effects is through a noncommutativity of spacetime coordinates. In the literature, there is not a clear way to describe at the same time a noncommutativity of spacetime and the phase-space noncommutativity of quantum mechanics. In this paper we address this issue by constructing a Drinfel'd twist in phase space which deals with both quantizations. This method can be applied to a noncommutativity which involves only space, leaving time aside. We apply our construction to the so-called λ-Minkwoski and R3λ noncommutative 

                          a. coordinates     b. candidates     c. effects      d. spaces.

Q55. arXiv:2112.12155 [astro-ph.SR]:  Wed, 22 Dec 2021 19:00:00 UTC (119 KB): [Submitted on 22 Dec 2021]: A Stringent Test of Magnetic Models of Stellar Evolution. Guillermo Torres (1), Gregory A. Feiden (2), Andrew Vanderburg (3), Jason L. Curtis (4) :ABSTRACT: Main-sequence stars with convective envelopes often appear larger and cooler than predicted by standard models of stellar evolution for their measured masses. This is believed to be caused by stellar activity. In a recent study, accurate measurements have been published for the K-type components of the 1.62 day detached eclipsing binary EPIC 219511354, showing the radii and temperatures for both stars to be affected by these discrepancies. This is a rare example of a system in which the age and chemical composition are known, by virtue of being a member of the well-studied open cluster Ruprecht 147 (age ∼ 3 Gyr, [Fe/H] = +0.10). Here we report a detailed study of this system with non-standard models incorporating magnetic inhibition of convection. We show that these calculations are able to reproduce the observations largely within their uncertainties, providing robust estimates of the strength of the magnetic fields on both stars: 1600±130 G and 1830±150 G for the primary and secondary, respectively. Empirical estimates of the magnetic field strengths based on the measured X-ray luminosity of the system are roughly consistent with these predictions, supporting this mechanism as a possible explanation for the radius and temperature 

                      a. variaations   b. discrepancies    c. reorded     d. distortions.. 

Q56. arXiv:2112.12611 [astro-ph.HE]: Thu, 23 Dec 2021 14:55:14 UTC (5,737 KB)[Submitted on 23 Dec 2021]: New approaches for faint source detection in hard X-ray surveys. V. A. Lepingwell, A. J. Bird, S. R. Gunn. :ABSTRACT: We demonstrate two new approaches that have been developed to aid the production of future hard X-ray catalogs, and specifically to reduce the reliance on human intervention during the detection of faint excesses in maps that also contain systematic noise. A convolutional neural network has been trained on data from the INTEGRAL/ISGRI telescope to create a source detection tool that is more sensitive than previous methods, whilst taking less time to apply to the data and reducing the human subjectivity involved in the process. This new tool also enables searches on smaller observation timescales than was previously possible. We show that a method based on Bayesian reasoning is better able to combine the detections from multiple observations than previous methods. When applied to data from the first 1000 INTEGRAL revolutions these improved techniques detect 25 sources (about 5% of the total sources) which were previously undetected in the stacked images used to derive the published catalog made using the same 

                                     a. format   b. dataset   c. data   d. noise.

Q57. arXiv:2112.12686 [hep-ph]: Thu, 23 Dec 2021 16:28:47 UTC (452 KB): [Submitted on 23 Dec 2021]: Classical and Quantum Evolution in a Simple Coherent Neutrino Problem. Joshua D. Martin, A. Roggero, Huaiyu Duan, J. Carlson, V. Cirigliano: ABSTRACT:The extraordinary neutrino flux produced in extreme astrophysical environments like the early universe, core-collapse supernovae and neutron star mergers may produce coherent quantum neutrino oscillations on macroscopic length scales. The Hamiltonian describing this evolution can be mapped into quantum spin models with all-to-all couplings arising from neutrino-neutrino forward scattering. To date many studies of these oscillations have been performed in a mean-field limit where the neutrinos time evolve in a product state. In this paper we examine a simple two-beam model evolving from an initial product state and compare the mean-field and many-body evolution. The symmetries in this model allow us to solve the real-time evolution for the quantum many-body system for hundreds or thousands of spins, far beyond what would be possible in a more general case with an exponential number (2N) of quantum states. We compare mean-field and many-body solutions for different initial product states and ratios of one- and two-body couplings, and find that in all cases in the limit of infinite spins the mean-field (product state) and many-body solutions coincide for simple observables. This agreement can be understood as a consequence of the fact that the typical initial condition represents a very local but dense distribution about a mean energy in the spectrum of the Hamiltonian. We explore quantum information measures like entanglement entropy and purity of the many-body solutions, finding intriguing relationships between the quantum information measures and the dynamical behavior of simple physical

                                      a. facts    b. rules    c. data     d. observables.

Q58. arXiv:2112.12686 [hep-ph]: Thu, 23 Dec 2021 16:28:47 UTC (452 KB): [Submitted on 23 Dec 2021]: Classical and Quantum Evolution in a Simple Coherent Neutrino Problem. Joshua D. Martin, A. Roggero, Huaiyu Duan, J. Carlson, V. Cirigliano: ABSTRACT:The extraordinary neutrino flux produced in extreme astrophysical environments like the early universe, core-collapse supernovae and neutron star mergers may produce coherent quantum neutrino oscillations on macroscopic length scales. The Hamiltonian describing this evolution can be mapped into quantum spin models with all-to-all couplings arising from neutrino-neutrino forward scattering. To date many studies of these oscillations have been performed in a mean-field limit where the neutrinos time evolve in a product state. In this paper we examine a simple two-beam model evolving from an initial product state and compare the mean-field and many-body evolution. The symmetries in this model allow us to solve the real-time evolution for the quantum many-body system for hundreds or thousands of spins, far beyond what would be possible in a more general case with an exponential number (2N) of quantum states. We compare mean-field and many-body solutions for different initial product states and ratios of one- and two-body couplings, and find that in all cases in the limit of infinite spins the mean-field (product state) and many-body solutions coincide for simple observables. This agreement can be understood as a consequence of the fact that the typical initial condition represents a very local but dense distribution about a mean energy in the spectrum of the Hamiltonian. We explore quantum information measures like entanglement entropy and purity of the many-body solutions, finding intriguing relationships between the quantum information measures and the dynamical behavior of simple physical

                                      a. facts    b. rules    c. data     d. observables.

Q59. The Modified Anti-Compton like Diagram with a TRUNK and co-joined by a joint propagator and with an outlined NEW formulation by Prof. Dr. Kotcherlakota Lakshmi Narayana, Phone. 09491902867. :ABSTRACT: The simplest diagram, depicting the blobs co-joined, by a joint propagator q and the TRUNK extending from the set (given below)

                             a. Anti Compton  b. Anti Dope   c. Compton   d. Modified 

Q60. arXiv:2112.12991 [hep-ph]: Fri, 24 Dec 2021 08:25:47 UTC (186 KB):[Submitted on 24 Dec 2021]: Some features of the direct and inverse double Compton effect as applied to astrophysics. Authors: V. Dubrovich, T. Zalialiutdinov. [ You may also refer my article "The Modified Anti-Compton like Diagram with a TRUNK and co-joined by a joint propagator and with an outlined NEW formulation by Prof. Dr. Kotcherlakota Lakshmi Narayana, Phone. 09491902867"] :ABSTRACT: In the present paper, we consider the process of inverse double Compton (IDC) scattering in the context of astrophysical applications. It is assumed that the two hard X-ray photons emitted from an astrophysical source are scattered on a free electron and converted into a single soft photon of optical range. Using QED S-matrix formalism for the derivation of a cross-section of direct double Compton (DDC) and assuming detailed balance conditions we give an analytical expression for the cross-section of the IDC process. It is shown that at fixed energies of incident photons the inverse cross-section has no infra-red divergences and its behavior is completely defined by the spectral characteristics of the photon source itself, in particular, by the finite interaction time of radiation with an electron. Thus, even for the direct process, the problem of resolving infrared divergence actually refers to a real physical source of radiation in which photons are never actually plane waves. As a result the physical frequency profile of the scattered radiation for direct as well as inverse double Compton processes is a function of both the intensity and line shape of the incident photon 

                             a. structure    b. ramification  c. field   d. expression.

Q61. arXiv:2112.14251 [physics.optics]: Tue, 28 Dec 2021 18:39:49 UTC (1,419 KB): [Submitted on 28 Dec 2021]: Optical synthesis by spectral translation. Authors: Jennifer A. Black, Zachary L. Newman, Su-Peng Yu, David R. Carlson, Scott B. Papp: ABSTRACT: Optical-frequency synthesizers are lasers stabilized and programmed from a microwave clock for applications, especially in fundamental measurements and spectroscopy, optical-communication links, and precision sensing of numerous physical effects. In a synthesizer, a frequency comb provides a reference grid across a broad spectrum and a frequency-tunable laser accomplishes synthesis by phase-lock to the comb. Optical synthesizers have matured to chip-scale with integrated photonics, however, the tunable laser and frequency comb fundamentally constrain the tuning range. Here, we present an optical synthesizer based on four-wave mixing (FWM) spectral translation of a tunable laser and a frequency comb. We implement both the spectral translation and the frequency comb by use of advanced microresonators. The intrinsic energy conservation of FWM ensures deterministic optical synthesis, and it allows a nearly arbitrary frequency tuning range by the dependence of resonant FWM on group-velocity dispersion, temperature, and tunable laser frequency. Moreover, we take advantage of highly efficient parametric amplification associated with spectral translation. We operate spectral translation across output ranges up to 200 THz, and we characterize it through ultraprecise optical-frequency metrology, demonstrating <0.1 Hz absolute accuracy and a fractional frequency precision of 4.7x10^(-13) in 1 s measurements. Our experiments introduce integrated-nonlinear-photonic circuits that enable complex intrinsic functionalities, such as our approach to optical-frequency synthesis with nearly limitless 

                         a.translation b.bandwidth  c.accuracy  d. frequency.  

Q62.arXiv:2112.13938 [gr-qc]:  Mon, 27 Dec 2021 23:36:16 UTC (12 KB): [Submitted on 27 Dec 2021]: Generalised Uncertainty Relations and the Problem of Dark Energy. Matthew J. Lake:ABSTRACT: We outline a new model in which generalised uncertainty relations, that govern the behaviour of microscopic world, and dark energy, that determines the large-scale evolution of the Universe, are intrinsically linked via the quantum properties of space-time. In this approach the background is treated as a genuinely quantum object, with an associated state vector, and additional fluctuations of the geometry naturally give rise to the extended generalised uncertainty principle (EGUP). An effective dark energy density then emerges from the field that minimises the modified uncertainty relations. These results are obtained via modifications of the canonical quantum operators, but without modifications of the canonical Heisenberg algebra, allowing many well known problems associated with existing GUP models to be 

                     a. erraneous   b. differed   c. universal   d. circumvented

+++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++++

TRUWIZ 123:  Dated: 9/9/2022 at 6:12 AM

Q1b,Q2a,Q3d,Q4c,Q5b,Q6a,Q7c,Q8a,Q9c,Q10a,Q11d,Q12b,Q13d,Q14a,Q15b,Q16c,Q17a,Q18c,Q19b,Q20d,Q21b,Q22d,Q23c,Q24a,Q25c,Q26b,Q27d,Q28a,Q29c,Q30a,Q31b,Q32d,Q33b,Q34d,Q35a,Q36c,Q37b,Q38a,Q39c,Q40b,Q41d,Q42b,Q43b,Q44a,Q45c,Q46d,Q47a,Q48b,Q49d,Q50b,Q51c,Q52a,Q53c,Q54d,Q55b,Q56b,Q57d,Q58d,Q59a,Q60c,Q61b,Q62d.

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